Untitled - Laboratoire d'Astrophysique de l'Observatoire de Grenoble

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12.2 Optical interferometry As for adaptive optics, part of the projects, as proposed below, have already started in the current ”quadrennial contract” or are extension of previous works into a more advanced phase. From our priorities described before, they will be preferentially directed towards imaging interferometry and nulling interferometry, taking benefit from the integrated optics advances in which LAOG has taken a large part. 12.2.1 Instruments PRIORITIES Imaging interferometry In some years, optical interferometry routine imaging will be one of the major achievements in astronomical instrumentation. The LAOG is strongly promoting this view and therefore is making steps towards this accomplishment. • VITRUV for the VLTI The LAOG has developed a proposition for a second generation VLTI instrument, VITRUV, that is aimed at imaging with 4 at start, 8 at maximum, telescopes offering a huge improvement in the u,v-plane coverage over AMBER. Its concepts takes benefit from the experience acquired with the tests of IONIC on IOTA and VLTI and is precisely oriented toward the main priority of ESO known as the ”4x4 VLTI box” that calls for 4 or more recombined telescopes, with phase reference allowing true imaging on faint sources. The project has passed a pre-phase A study and has been proposed to ESO in April 2005 (see section 11.2.3). Since then, the LAOG is implicitly committed to VITRUV in terms of key-responsabilities, design, integration, tests and commissioning and is awaiting the ESO decision to start the phase-A study. As AMBER was, this project would be an international collaboration. Several European partners have expressed their interest in participating to the project at various levels. It must be noted that, due to its concept, VITRUV should require slightly less resources than AMBER. • CHARA : participation to the instrumentation In the path to VITRUV, we have developed strong ties with Pr. Monnier at U. of Michigan in order to test key VITRUV building blocks on a real on-sky imaging experiment. The MIRC imaging instrument of CHARA is fully compatible with LAOG integrated optics beam combiners and offers a unique opportunity to demonstrate VITRUV imaging capability. The eventuality to leave useful components for inclusion in a CHARA general-User instrument such as MIRC is an open question. OPTIONAL PROJECTS The following projects are either space projects or dedicated to Antarctica. Because of our available resources, the LAOG contribution can only be kept limited if VITRUV is launched as we do hope. But if it was not, our contribution could probably be increased since our interest in these projects is important. • PEGASE and/or DARWIN space missions LAOG is directly involved in the PEGASE project which was presented at the French CNES space agency as an answer to the Call-for-proposal for a free-flyers mission and is now a candidate for a Phase A study. At this stage, LAOG contributes to the scientific drivers definition (study of gaps in protoplanetary disks and spectroscopic characterization of hot Jupiters). Later on, LAOG could have a technical participation in the global conceptual design and the recombining aspects if IO is retained as a solution. The involvement in PEGASE is not only motivated by standalone objectives but also by the will to participate to the very challenging mission DARWIN that we have been preparing by several R&D related to DARWIN (see Sect. 11.2.4), under ESA contracts. In the event where PEGASE were not selected for a phase-A study, our involvement in the R&D preparation to DARWIN would however be maintained because of the needs for a long-term approach to this most challenging mission. • Antarctica Genie-type projects Mark Swain (from JPL) spent one year in LAOG to work on exploitation of AMBER and Antarctic interferometry. On this last subject, the LAOG has helped him to present the problematics of Antarctic interferometry throughout Europe. Also thanks to the fruitful links between the 132
laboratories of OSUG, a collaboration has grown up between LAOG and LGGE (H. Gallee) on the climate modelling in Antarctica to model astronomical seeing, demonstrating the importance of the boundary layer in Antarctica, of the order of 20-30 m high. The result is that seeing above this layer is exceptionally good almost like space conditions, but at the ground level it is rather similar to other sites. Work has started to use these results to predict performances of future instruments in Antarctica thanks to the experience developed at LAOG for the AMBER instrument. Preparatory activities in view of astronomical use of the Dome C Site in Antarctica have been largely reinforced early 2005 with various medium-size equipment funding requests (to INSU/CSA and/or to IPEV) by several French laboratories and a European FP6 funding request led by N. Epchtein (LUAN), aiming at promoting first level studies of astronomical use of the Dome C, whose funding would cover the period 2006-2007 and whose rationale must also be found in the preparation of a large scale FP7 proposal. In this context, LAOG is involved in the FP6 request at a limited level (6 men-months with 4 involved persons) with the aim to participate in the definition of the astronomical goals and the studies of the instrumental optimization for the Antarctica environment. We intend in particular to bring our expertise in integrated optics interferometric recombiners and in interferometry at a system level. In parallel, the LAOG may wish to look into the potentially major interest that GENIE, or an other nulling instrument like ALLADIN, be installed at Dome C rather than on the VLTI and the compared figures of merit to install 8m-type telescopes at Dome C as an alternative to ELTs on standard sites. We intend to participate in the conceptual studies on which future decisions will have to be based. 12.2.2 Software development for interferometry JMMC and European networks The detailed objectives of JMMC for this period will be described in the report and request for renewal that will be prepared by the JMMC as a CNRS GdR (their preliminary presentation is given in Appendix 2). We describe here how we feel, at LAOG, the orientation of the JMMC should be for the next years. The JMMC is currently heavily loaded by the tasks assigned by its council to which its participation, as a major actor, to the Opticon JRA4 has added further pressure in 2004. Its present main guideline is to develop software for the end Users of interferometry. The scheduled tasks include the development of software specific to the optimized use of AMBER and it can be anticipated that the JMMC will try to cover the new needs induced by the forthcoming installation of VITRUV-type (i.e. imagers) instruments on the VLTI. Moreover, optical interferometry already joined other observational techniques in the more general framework of virtual astronomical observatories, bringing some more constraints to the work load of JMMC. In the future, the development of JMMC should be pursued with in mind an easy access to interferometric data by the general astronomers both for preparing observations and for reducing them or access to science archives. In this respect, a major outcome of JMMC is the possibility to produce and offer an image reconstruction software optimized for aperture synthesis by optical interferometry. With all these undertakings, the JMMC is very likely to be continued by CNRS for at least the length of the new ”quadrennial contract”. In the longer term, it must be added that it could be beneficial to the community that the JMMC extend its activities (services and support) to the larger domain of all high angular resolution techniques i.e. including the specific AO data expected with ELTs. 12.2.3 R&D activities PRIORITIES Advanced IO components development In the domain of near-IR IO, the basic recombining functionalities are now rather well mastered at least for 3 telescopes recombination. Future progress will come from more functionally complex components, i.e. allowing recombination of more than 3 beams, or providing not yet integrated functions like fringe tracking, achromatic phase shift or active functions (e.g. OPD scanning). Such components would further strengthen the advantages of IO-based interferometric benches, therefore decrease the overall system costs, a particularly interesting prospect for space applications. As we did before with IOTA, we intend to test the components previously characterized in the laboratory on the CHARA interferometer (Georgia State University) whose size and access are more adapted to this goal than 133
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LABORATOIRE D’ASTROPHYSIQUE DE GR
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III Team ASTROMOL 41 2 Presentation
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8.1.3 Graduate Students . . . . . .
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VI Team SHERPA 145 15 Results 147 1
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Part I Foreword: Presentation of th
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Part II Executive Summary A 18th ce
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of CNRS for technicians and enginee
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Figure 1.3: New LAOG organigram (20
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heart attack. Manuel went back to t
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Figure 1.6: PhD student repartition
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• LAOG researchers (and publishin
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and published 95 papers in four yea
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• National astronomy programs. 4
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1.5 From dreams to reality: Human r
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and accretion disks with heavy nume
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emphasis on the chemistry of planet
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Part III TEAM ASTROMOL Sub-arcsecon
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• we develop quantum and classica
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Table shows not only the volume of
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• Herschel-HIFI: Astromol is invo
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particular, we calculated a 9D H2O-
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• The hot corinos. More spectacul
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the massive deeply embedded protost
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tens of visual magnitudes, hence pr
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quantum VCC-IOS approximation may f
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Rate constant (cm 3 s -1 ) 1e-09 1e
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• One of us (PV) is strongly invo
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sublimation of water ice trapped ei
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If the chemistry in the first phase
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4.2.2 Molecular Physics The theoret
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Source Herschel Time Astromol Class
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several important studies that anti
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Chapter 5 Selected Publications •
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Part IV TEAM FOST The first image o
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393254 (5MJup at 55 AU) & AB Pic (1
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